Atmospheric velocity fields in tepid main sequence stars

Details Atmospheric velocity fields in tepid main sequence stars Atmospheric velocity fields in tepid main sequence stars

2009-06-20

arxiv.org/abs/0906.3824v1

Astronomy and Astrophysics, vol. 503, 973 (2009)

Astronomy and Astrophysics

Astrophysics

Solar and Stellar Astrophysics

Acepted for publication by Astronomy and Astrophysics

Scientific paper

10.1051/0004-6361/200912083

The line profiles of the stars with v sin i below a few km/s can reveal direct signatures of local velocity fields (e.g. convection) in stellar atmospheres. This effect is well established in cool main sequence stars, and has been detected and studied in three A stars. This paper reports observations of main sequence B, A and F stars with two goals: (1) to identify additional stars having sufficiently low values of v sin i to search for spectral line profile signatures of local velocity fields, and (2) to explore how the signatures of the local velocity fields in the atmosphere depend on stellar parameters such as effective temperature T_eff and peculiarity type. For stars having T_eff below about 10000 K, we always detect local atmospheric velocity fields indirectly through a non-zero microturbulence parameter, but not for hotter stars. Among the A and F stars in our sample having the sharpest lines, direct tracers of atmospheric velocity fields are found in six new stars. The velocity field signatures identified include asymmetric excess line wing absorption, deeper in the blue line wing than in the red; line profiles of strong lines that are poorly fit by computed profiles; and strong lines that are broader than they should be for the v sin i values deduced from weak lines. These effects are found in both normal and Am stars, but seem stronger in Am stars. These data still have not been satisfactorily explained by models of atmospheric convection, including numerical simulations.

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